Post on 10-Feb-2018
Clustering and evolution of radio, X-ray, and IR-selected AGN
Ryan C. Hickox
Harvard-SmithsonianCenter for Astrophysics
SDSS SymposiumChicago, IL
15 August 2008
Collaborators on9 deg2 Boötes survey
Chandra (CfA)C. JonesW. FormanS. MurrayA. KenterR. Narayan
Optical photometry (NOAO/etc.)B. JanuzziA. DeyK. BrandM. Brownand the NDWFS Team
Spitzer IRAC (JPL/Caltech/CfA)P. EisenhardtM. BrodwinV. GorjianD. SternM. Pahreand the IRAC Shallow Survey Team
Optical spectroscopy (OSU/Arizona/CfA)K. KochanekD. EisensteinR. CoolN. Caldwelland the AGES Team
The AGN and Galaxy Evolution Survey
Hectospec on MMT used to obtain ~20,000 galaxy
redshifts over 7.3 deg2 to z ~ 0.8
~2,000 AGN redshifts
Complementary to
very wide/shallow
(e.g., SDSS) and
narrow/deep (e.g.,
DEEP2) redshift
surveys
The AGN and Galaxy Evolution Survey
Hectospec on MMT used to obtain ~20,000 galaxy
redshifts over 7.3 deg2 to z ~ 0.8
~2,000 AGN redshifts
Complementary to
very wide/shallow
(e.g., SDSS) and
narrow/deep (e.g.,
DEEP2) redshift
surveys
0.25 < z < 0.8
AGN feedback may needed to quench star formation and form the red sequence(e.g., Hopkins et al. 2006, Croton et al. 2006, Rafferty et al. 2008)
Black hole and bulge properties are tightly related(e.g., Magorrian et al. 1998, Ferrarese & Merritt 2000, Gebhart et al. 2000, Tremaine et al. 2002)
Links between AGN & galaxy evolution
Growing evidence for multiple AGN accretion modes“quasar” vs. “radio”(e.g., Churazov et al. 2005, Merloni & Heinz 2008, Somerville et al. 2008)
Questions we ask
What modes of AGN
accretion are found at “low”
redshift (z ~ 0.5), and how do
they depend on host galaxy
properties and environment?
Questions we ask
What modes of AGN
accretion are found at “low”
redshift (z ~ 0.5), and how do
they depend on host galaxy
properties and environment?
How does what we see at
z ~ 0.5 relate to our general
picture of galaxy and AGN
evolution?
How we answer them
How we answer them
Select AGNs at multiple
wavelengths for a (more)
complete AGN sample
1) Host galaxy propertieshost masses, stellar populations
2) Eddington ratiosfueling, accretion modes
3) Spatial correlationsenvironments, DM halo mass
How we answer them
Select AGNs at multiple
wavelengths for a (more)
complete AGN sample
1) Host galaxy propertieshost masses, stellar populations
2) Eddington ratiosfueling, accretion modes
3) Spatial correlationsenvironments, DM halo mass
How we answer them
Select AGNs at multiple
wavelengths for a (more)
complete AGN sample
Compare to theoretical
evolutionary picture
Boötes AGN selection
~6000 galaxies and 600 AGN with AGES redshifts at 0.25 < z < 0.8
Boötes AGN selection
~6000 galaxies and 600 AGN with AGES redshifts at 0.25 < z < 0.8
P1.4 GHz > 5 x 1023 W Hz-1
Boötes AGN selection
All X-ray sourcesLX > 1042 ergs s-1
~6000 galaxies and 600 AGN with AGES redshifts at 0.25 < z < 0.8
P1.4 GHz > 5 x 1023 W Hz-1
Boötes AGN selection
All X-ray sourcesLX > 1042 ergs s-1
Color-color selection (Stern et al. 2005)
~6000 galaxies and 600 AGN with AGES redshifts at 0.25 < z < 0.8
P1.4 GHz > 5 x 1023 W Hz-1
(1) AGN host galaxies
Focus on AGN with extended optical counterparts (AGN is either intrinsically faint or obscured)
(1) AGN host galaxies
• Radio AGN live in luminous red galaxies
(1) AGN host galaxies
• Radio AGN live in luminous red galaxies• X-ray AGN are found preferentially in the “green valley” (see also Nandra et al. 2007, Silverman et al. 2007, Alonso-Hererro et al. 2008, Georgakakis et al. 2008)
(1) AGN host galaxies
• Radio AGN live in luminous red galaxies• X-ray AGN are found preferentially in the “green valley” (see also Nandra et al. 2007, Silverman et al. 2007, Alonso-Hererro et al. 2008, Georgakakis et al. 2008)
• Infrared AGN are primarily found in blue cloud galaxies
(2) Eddington ratios
(2) Eddington ratios
(2) Eddington ratios
Radio:Lbol/LEdd < 10-3
X-ray:10-3 < Lbol/LEdd < 1
IRAC:Lbol/LEdd > 10-2
courtesy S. Murray
(3) AGN clustering
courtesy S. Murray
(3) AGN clustering
courtesy S. Murray
(3) AGN clustering
DARK MATTER HALO?
courtesy S. Murray
Clustering measurements give us estimates of dark matter halo mass
Interesting fact: broad-line quasars reside in
DM halos of constant mass, (~3 x 1012 M☉ ) to z ~ 4 (e.g., Croom et al. 2005, Coil et al. 2007, Myers et al. 2007, Shen et al. 2007)
(3) AGN clustering
Correlation results
Correlation results
Galaxies show dependence on clustering with host galaxy color (as in SDSS, DEEP2, 2dFGRS, etc.)
AGN-galaxy cross-correlation
Radio AGN are strongly clustered (b = 2.4)
Mhalo ~ 5 x 1013 h-1 M☉
AGN-galaxy cross-correlation
Radio AGN are strongly clustered (b = 2.4)
X-ray AGN are clustered like a typical AGES galaxy (b = 1.5) Mhalo ~ 1013 h-1 M☉
AGN-galaxy cross-correlation
Radio AGN are strongly clustered (b = 2.4)
X-ray AGN are clustered like a typical AGES galaxy (b = 1.5)
Infrared AGN are weakly clustered (b = 1.1)
Mhalo ~ 2 x 1012 h-1 M☉
The AGN census 0.25 < z < 0.8
Optically-faintX-ray AGN
Optical/IRSeyfert galaxy
Radio AGN
The AGN census 0.25 < z < 0.8
Optically-faintX-ray AGN
Optical/IRSeyfert galaxy
Radio AGN
• Red host galaxies• Low Lbol/LEdd
• Large DM halos
(~ 5 x 1013 h-1 M☉)
The AGN census 0.25 < z < 0.8
Optically-faintX-ray AGN
Optical/IRSeyfert galaxy
Radio AGN
• Red host galaxies• Low Lbol/LEdd
• Large DM halos
(~ 5 x 1013 h-1 M☉)
• Green host galaxies• Moderate Lbol/LEdd
• Medium DM halos
(~ 1013 h-1 M☉)
The AGN census 0.25 < z < 0.8
Optically-faintX-ray AGN
Optical/IRSeyfert galaxy
Radio AGN
•Blue host galaxies•High Lbol/LEdd
•Small DM halos
(~ 2 x1012 h-1 M☉)
• Red host galaxies• Low Lbol/LEdd
• Large DM halos
(~ 5 x 1013 h-1 M☉)
• Green host galaxies• Moderate Lbol/LEdd
• Medium DM halos
(~ 1013 h-1 M☉)
Initial halo mass (and clustering bias)
High Medium
SMG/ULIRG
Optical/IR quasar
Optically-faintX-ray AGN
Early-type galaxy
Radio galaxy
Early-type galaxy
Disk galaxy(s)
Low
Co
smic
time
z ~ 4
z ~ 1
z ~ 0
(an
d h
alo
ma
ss)
Mh
alo
~ 1
012 -
1013
M☉
A cartoon model for AGN evolution
Initial halo mass (and clustering bias)
High Medium
SMG/ULIRG
Optical/IR quasar
Optically-faintX-ray AGN
Early-type galaxy
Radio galaxy
Early-type galaxy
Disk galaxy(s)
Low
Co
smic
time
z ~ 4
z ~ 1
z ~ 0
(an
d h
alo
ma
ss)
Optically-faintX-ray AGN
Mh
alo
~ 1
012 -
1013
M☉
A cartoon model for AGN evolution
Initial halo mass (and clustering bias)
High Medium
SMG/ULIRG
Optical/IR quasar
Optically-faintX-ray AGN
Early-type galaxy
Radio galaxy
Early-type galaxy
Disk galaxy(s)
Low
Co
smic
time
z ~ 4
z ~ 1
z ~ 0
(an
d h
alo
ma
ss)
Optical/IR Seyfert galaxyOptically-faint
X-ray AGN
Mh
alo
~ 1
012 -
1013
M☉
A cartoon model for AGN evolution
Initial halo mass (and clustering bias)
High Medium
SMG/ULIRG
Optical/IR quasar
Optically-faintX-ray AGN
Early-type galaxy
Radio galaxy
Early-type galaxy
Disk galaxy(s)
Low
Co
smic
time
z ~ 4
z ~ 1
z ~ 0
(an
d h
alo
ma
ss)
Optical/IR Seyfert galaxy
Observed at0.25 < z < 0.8
Optically-faintX-ray AGN
Mh
alo
~ 1
012 -
1013
M☉
A cartoon model for AGN evolution
The future
The future • Compare observables
to more detailed model
predictions
• Relate AGN accretion
modes to host galaxy
physical properties such
as mass & SF history (see forthcoming paper on AGN in
post-starburst galaxies by Brown et
al.)
• Direct evidence for
AGN /galaxy interaction?